[1]} focused on a sample of 59 binary systems with at least one RG component, which had been characterized by [2]}, [3]}, [4]}, and [5]}, [6]}. [1]} tested the equilibrium tideThe equilibrium tide is the large-scale flow induced by the hydrostatic adjustement of a star induced by the presence of a companion [8]}, [9]}. This flow is completed by the so-called dynamical tide [10]}, which is constituted by oscillation eigenmodes that are excited by the tidal force, that is, tidal gravity waves in stably stratified radiation zones [10]} and tidal inertial waves in convective regions [12]}. model of [8]}, [14]}, [15]}, [16]} by investigating if the eccentricity variations predicted by these theoretical calculations allowed them to explain the orbital eccentricity distribution in their sample. [1]} found a good agreement between theory and observations, which we explain in more detail in the next paragraphs. The approaches of [18]} and [1]} are complementary because they implemented observational tests of the tidal theoretical results through two independent methods. In this subsection, we explain why the 16 binaries characterized in this workThat is, all our sample except from KIC 4473933. complete the sample of 59 systems of [1]}.
